Keck Next Generation Adaptive Optics
KAON 571
NGAO Observing Scenarios
Draft Version 1.0
D. Le Mignant1,
E. McGrath2, C. E. Max2
2.
1.
1.
W. M. Keck Observatory
Center for Adaptive Optics, University California Santa Cruz
INTRODUCTION.............................................................................................................................................................. 3
1.1.
1.2.
1.3.
2.
PURPOSE OF THE DOCUMENT ......................................................................................................................................... 3
REFERENCES .................................................................................................................................................................. 3
ACRONYMS AND ABBREVIATIONS .................................................................................................................................. 3
INTRODUCTION TO OBSERVING WITH NGAO ..................................................................................................... 3
2.1.
2.2.
2.3.
2.4.
2.5.
3.
OBSERVING MODEL........................................................................................................................................................ 3
SCIENCE OPERATIONS TOOLS ......................................................................................................................................... 3
NGAO ACQUISITION SEQUENCE .................................................................................................................................... 4
OBSERVING SEQUENCES: DITHER AND OFFSET ............................................................................................................... 5
OBSERVING EFFICIENCY BUDGET ................................................................................................................................... 6
GALAXY ASSEMBLY AND STAR FORMATION HISTORY ................................................................................... 7
3.1. OBSERVING STRATEGY AND OBSERVING EFFICIENCY: ................................................................................................... 7
3.2. PRE-OBSERVING PLANNING:........................................................................................................................................... 9
3.3. AO OBSERVING MODE: .................................................................................................................................................. 9
3.4. SCIENCE INSTRUMENT CONFIGURATION:........................................................................................................................ 9
3.5. OBSERVING SEQUENCES: ............................................................................................................................................. 10
3.5.1. Acquisition ........................................................................................................................................................... 10
3.5.2. Science observing sequences................................................................................................................................ 10
3.6. SCIENCE CALIBRATIONS: ............................................................................................................................................. 11
3.7. POST-OBSERVING ........................................................................................................................................................ 11
4.
NEARBY ACTIVE GALACTIC NUCLEI ................................................................................................................... 11
5. PRECISION ASTROMETRY: MEASUREMENTS OF GENERAL RELATIVITY EFFECTS IN THE
GALACTIC CENTER ............................................................................................................................................................ 11
6.
IMAGING AND CHARACTERIZATION OF EXTRASOLAR PLANETS AROUND NEARBY STARS ........... 11
7.
MULTIPLICITY OF MINOR PLANETS .................................................................................................................... 12
8.
QSO HOST GALAXIES ................................................................................................................................................. 12
9.
GRAVITATIONAL LENSING ...................................................................................................................................... 12
10.
ASTROMETRY SCIENCE IN SPARSE FIELDS ..................................................................................................... 12
11.
RESOLVED STELLAR POPULATIONS IN CROWDED FIELDS ....................................................................... 12
12.
DEBRIS DISKS AND YOUNG STELLAR OBJECTS .............................................................................................. 12
13.
SIZE, SHAPE AND COMPOSITION OF MINOR PLANETS................................................................................. 12
14.
CHARACTERIZATION OF GAS GIANT PLANETS .............................................................................................. 12
15.
CHARACTERIZATION OF ICE GIANT PLANETS ............................................................................................... 12
16.
BACKUP SCIENCE ...................................................................................................................................................... 12
Last updated by D. Le Mignant
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Observing Scenarios with NGAO – Draft Version 1.0
List of Tables:
TABLE 1: GENERIC ACQUISITION STEPS FOR NGAO ..................................................................................................................... 5
TABLE 2: OBSERVING PARAMETERS FOR THE “GALAXY ASSEMBLY AND STAR FORMATION HISTORY” SCIENCE CASE .................. 8
List of figures:
FIGURE 1: ESTIMATED BUDGET FOR THE OBSERVING EFFICIENCY ................................................................................................ 7
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1. Introduction
1.1. Purpose of the document
As part of the NGAO System Design phase (KAON 414), the NGAO Science Case Requirements have been presented and
discussed in KAON 455 while KAON 548 provided the summary table in support of system architecture evaluations.
The purpose of this report is to complement KAON 455 and 548 and document the observing scenarios for the NGAO
Science Cases for both the Key Science Drivers and Science Drivers.
1.2. References
- KAON 455: In the following sections, the references to the KAON 455 requirements are noted in italic e.g., (reqt #1.2)
refers to the science case requirement #1.2 found in the KAON 455 tabulated requirements.
- KAON 548 presents a summary for the science requirements in support of the architecture evaluations.
- KAON 456: The requirements for the science operations are described in the NGAO System Requirement Document
(SRD – KAON 456) under two sections: Sec. 6.1.4 for Science Operations Requirements from the Science Cases and
Sec. 6.2.5 for the Observatory Operational Requirements.
- KAON 476 presents a trade study on the observing models for Keck NGAO.
- In developing the observing scenarios, we have made some assumptions based on the lessons learned for LGS operations
at Keck (KAON 463). Particularly:
- the fraction of LGS science time lost to weather is 25%.
- only 55% of the nights year-round are considered fully photometric
- the software architecture will allow for parallel operations of subsystems, reducing the overall overhead
1.3. Acronyms and abbreviations
The following acronyms and abbreviations are used in this document:
- KAON: Keck Adaptive Optics Notes, available from the NGAO Twiki site or from KeckShare
- NGS: Natural Guide Star
- LGS: Laser Guide Star
- TAC: Time Allocation Committee
- LOWFS: Low Order Wavefront Sensor, sensors looking at a NGS used for tip-tilt / focus and astigmatism.
- TWFS: True Wavefront Sensor, sensor looking at a NGS used for providing a true reference for the average residual
aberrations.
- d-IFS: deployable Integral Field Spectrograph
- IFU: Integral Field Unit
2. Introduction to observing with NGAO
This section is intended to provide some background information on the NGAO science operations at the W. M. Keck
Observatory.
2.1. Observing model
The paradigm for the NGAO science operations is to optimize the observing efficiency with the astronomer(s) being in
control of the observations with the technical support of Keck staff. NGAO will be operated in classical observing mode
with the possible option of implementing flexibility in the schedule per TAC (KAON 476).
2.2. Science operations tools
The science operations tools for NGAO include a suite of tools:
I. the planning tools to: 1) search and select the AO Natural Guide Stars, 2) compute and predict AO performance, 3)
prepare the observing sequences, 4) estimate the exposure time and 5) estimate the observing efficiency.
II. the observing sequences control (OSC) tools to: 1) load, 2) check, 3) command and 3) view the observing sequences
for the AO and the science instruments. These include Users’ Interfaces and Execution Modules for the astronomer
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and the observing support personnel. These tools are high-level command tools and coordinate the actions of the
sequencer for each subsystem (Science Instrument, Telescope, AO, Laser, Data Server, etc).
III. the post-observing tools to: 1) select the data to save, 2) provide an estimate for the PSF calibrations (including PSF
reconstruction) and 3) archive data when applicable.
The science operations tools will be detailed elsewhere during the NGAO design phases (TBD).
2.3. NGAO acquisition sequence
Three types of targets needs to be acquired on the NGAO photo-sensors:
- the NGS for the LOWFS, the TWFS and/or the WFS
- the astronomical sources for the science instruments:
o for the d-IFS: target galaxies plus simultaneous science field calibrators
o for the narrow field science instruments: the science target
- the Laser Guide Stars for the HO WFS.
The LGS acquisition section will be detailed in the next iterations of the observing scenarios, depending of the options
selected for the LGS asterisms and the point-and-shoot mode.
The table below presents a generic description for the acquisition sequence (see KAON 567).
Step
Observing Step
Parallel Steps
Remarks
0
Select next target:
- assess science priority
- check target elevation range
- check observing conditions
- check LTCS conditions
Complete integration on current
science target or calibrator.
When target selected from Planning
Tools, then information is loaded in
OSC Tools.
It is not clear yet whether
the astronomer will have
to run these checks
manually or whether it
will be automated.
1
Upon completion of readout of science
array, LGS is shuttered, AO loops open
and key-system feedback parameters are
saved then the Science Operations
(ScOp) Tools triggers the telescope
slew.
Telescope slews
OSC Tools parses information, and
get ready for execution:
- NGS parameters for
acquisition
- AO configuration
- Instrument configuration
The OSC Tools sends command to
the subsystem sequencer and setup
sequences are executed as
appropriate by the AO, Laser,
Science Instrument subsequencers.
2
3
Telescope Pointing Adjustment on one
of the NGS (brightness allowing). This
steps is automatically performed by the
NGS acquisition subsystem with the
visual check of the Observing Assistant
(OA). Upon success, pointing
corrections are applied and next
telescope slew is commanded from the
OSC.
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This step is required
when the NGS are fainter
than R=18 mag. (TBC)
or when the telescope
slews by more than x deg
in elevation/azimuth
range.
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4
Telescope coarse registration on the
science field. NGS acquisition
subsystem runs an automated routine to
record and process image, ID the NGS
in the field wrt catalog data then
compute required offset. Visual check
of process by OA. Upon success,
position offsets are applied to telescope.
LGS propagation and acquisition
steps initiated.
If small telescope centering offset
(<5 “ – TBC), uplink TT correction
closed with very low gain.
Pickoff positioning and LOWFS
setup complete including
background.
Need to implement the
acquisition for the
vibration/wind shake
reference. Need addit’al
study for telescope
guiding. Not clear if the
HOWFS will require a
background.
5
Telescope fine registration on the
science field: If photons are not detected
at the expected SNR on the LOWFS (or
NGS not on Pointing Origin), then NGS
acquisition subsystem runs a second
iteration. Visual check of process by
OA.
Iterate if necessary (to be detailed).
Upon completion adjust telescope
pointing model.
AO subsystem control: 1) low gain on
woofer and MEMs, 2) increase gain on
UT, 3) start telescope guiding, 4) adjust
woofer and MEMs gain, 5) initiate
TWFS + tomography optimization
Pick-off mirrors for science and
TWFS in position
Need to check the
conditions for the
dichroic during this step.
Need to be able to adjust
pointing model for
telescope even though
PO != REF.
Science instrument is setup: optics
and read modes are set and
confirmed.
May record first exposure to check
centering with point-source and
expected SNR/coadd.
Monitor image quality and assess
optimization progress.
UTT control
(all/individual?)
Assuming redundant
information from
USNO-B, GSC-II and
SDSS, uncertainty in the
field centering should be
~0.2” (TBC).
6
7
Science integration starts
Table 1: Generic acquisition steps for NGAO
The main contributions to the centering error budget during NGAO acquisition in LGS mode are:
1. The accuracy for the knowledge of the separation distance and PA between the stars and the galaxies from the
literature. This information is provided by the astronomer, and can be less than 10 milli-arcsecond if the field has
been observed (recently) with HST cameras. The USNO-B on-line catalog provides an astrometric accuracy of 200
milli-arcsecond, and the astrometric solution for the USNO-B, GSC-II and SDSS catalogs are improved as the
proper motions are being calibrated using GSC-I (KAON 467).
2. The accuracy in positioning the pickoff arm for each science target w/ respect to the TT closed-loop reference
position for the LOWFS, which is the total of:
a. The internal positioning accuracy and position stability for each individual pick-off arm (science and
LOWFS) – the requirement is less than 5 milli-arcsecond (KAON 548)
b. Registration accuracy and stability between LOWFS and science arms including TT stage positioning
accuracy.
3. The differential atmospheric refraction between the LOWFS and the science
4. The total contribution from the optical distortions due to thermal gradient, alignment error, woofer and MEMs
positioning between the science array and the LOWFS.
KAON 559 provides a conceptual study report for the “Interim LOWFS and LGS Object Selection Mechanism” and shows
that the requirement for the positioning accuracy can be met (contribution #2 above). Yet, contribution # 3 and #4 will need
further analysis during the PD or DD phases.
2.4. Observing sequences: dither and offset
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The observing sequences will be coordinated at the Observing Sequence Tool level to minimize the overhead during dither
and offset scripts: as soon as the instrument reports that the readout is complete, the OS tool will command the dither or
offset either in instrument pixel or sky coordinates. KAON 558 proposes possible scenarios for dither and offset. We
anticipate that any repositioning of the observing reference frame of less than 5” (TBC) will be performed by repositioning
internal optics and will not require to move the telescope (hence not require to open any loops). These we propose to define
as “dither” and should take less than 5 seconds.
Conversely, any move that require to move the telescope and open the AO loops are defined as offset, and may require
longer overhead (~ 15 -30 sec - TBC).
2.5. Observing efficiency budget
We have developed a simple MS excel-based tool to estimate the observing efficiency for the NGAO science cases. Each
science case has its own spreadsheet where open shutter time and overhead have been estimated for the science target and the
calibration standard. We have made the following assumptions:
- Open shutter time on the sky-calibration (telluric and flux standards, sky background) is considered science time.
- The main contributors to the observing overhead will be the telescope slews, telescope pointing adjustment and field
registration, NGAO and science field acquisitions, fine centering and re-centering, dither/offset + instrument setup +
readout.
- For each contribution (open shutter and every overhead), we estimate the minimum, median and maximum values and
calculate a weighted average with the following weights (1/6, 4/6, 1/6).
- Estimates for the overhead contributions from telescope slews, pointing adjustments and NGS acquisitions are derived
from KAON 567.
- Additional overhead has been included for LTCS interrupts in form of an integer number of individual science
integration (hence a higher impact for long integration) and subsequent time for re-centering the science target(s). Note
that LTCS interrupts will be greatly reduced by the use of the “first-on-target” rule and the use of planning tools to
avoid science observing during planned interrupt request from the Laser Clearinghouse.
- The overhead for dither/offset will be reduced compared to the current system if we adopt a different strategy for
dither/offset (KAON 558)
No time loss has been included for NGAO system failure at this point as we know very little about the NGAO failure
rate. This could be considered overly optimistic, yet it is counterbalanced by the allocation of maximum values for
every overhead.
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Figure 1: Estimated budget for the observing efficiency
The Observing Efficiency Tool can be downloaded from:
http://www.oir.caltech.edu/twiki_oir/bin/view/Keck/NGAO/NGAOObservingScenarios
3. Galaxy assembly and star formation history
The NGAO Science Case on Galaxy Assembly and Formation History is one of the five Key Science Drivers, which place
the most restrictive or technologically challenging constrains on the NGAO system.
The requirements for this science case are described in Section 2.1.1 in KAON 455. The following sub-sections document
the observing scenarios.
3.1. Observing strategy and observing efficiency:
The observing goal for this science case is to survey more than 200 galaxies over a few years (reqt #1.2) . This is possible by
using a deployable NIR spectrograph over a field of ~ 2 arcmin diameter. The number of targets per field of regard depends
on the number density for the class of objects being studied and varies between 0.1 to 40 arcmin -2 (see KAON 455, table 3).
Depending on the object brightness, the NGAO + dIFS will dedicate ~ 1.5 to 4 hours of open shutter time on a set of targets
(reqt #1.2).
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Parameters
Science instrument
Instrument setup
Total integration time on
target
Individual integration
time on target
Individual integration
time on calibration stars
Positioning precision of
IFU with respect to the
NGS
Background estimation
Instrumental calibration
PSF calibration
Telluric standard
Dedicated background
Value
d-IFS
IFU FoV: 1 x 3 arcsec
J-K wavelength range
70 mas/spaxel
35 mas/pixel TBD
1.5 - 4 hours
Comments
reqt #1.2
15 - 30 min
20 - 60 sec
< 100 milli-arcsec
Dither on IFU
Using arc lamps and integrating
sphere
Using an IFU ?
goal of 20 milli-arcsec ?
between LOWFS arms and IFU
arms?
Observer are likely to use a
dithering script on the IFU
Performed during the day
Telemetry-based PSF
reconstruction
Using an IFU ?
Dedicated observing sequence
Yes, by offsetting off the IFU at
least once – TBD
Table 2: Summary of the observing parameters for the “galaxy assembly and star formation history” science case
In estimating the observing efficiency, we have made the following assumptions:
- In parallel to observing a set of extragalactic target, we anticipate the observer will dedicate one of the deployable units
on a point-like source to calibrate for the PSF, and possibly for the telluric absorption (depending on the spectral class
for the point-like source). This point-like source will also be used to monitor the centering of the field.
- Yet, for every set of targets, we anticipate the observer will calibrate for the telluric absorption after the science
spectroscopy observations and within a certain interval in air mass and time. This should add approximately 10 min of
observing time to the observations of the set of targets. In addition, we anticipate the observer will want to calibrate the
flux by observing flux standards, twice trough the night.
- We assumed individual integration time between 15 and 30 min on the d-IFS for the science targets and between 1 and 3
min for the standards.
- For an observation on a set of targets, we find that it will take 12 min on average for the full setup from initiating the
telescope slew till first start of science-quality exposure. The open shutter time will be 155 min on average with 3 min
of overheads for dither/readout and 5.3 min for re-centering. The observation of the telluric of flux standard will take
approximately 9 min including ~ 55% total overhead (telescope slew, acquisition, dither, readouts).
- We anticipate 27 min loss due to LTCS interrupts, mainly a consequence of the long integration time.
Using these assumptions, we derive that it will be possible to observe 3.14 science fields including the telluric standards and
two flux standards for an average night of 10.25 hours numbers.
The total observing efficiency (open shutter on science, including standards) is 83%.
Assuming 3, 5 and 6 deployable units used (minimum, median, maximum, respectively) on the science targets, this leads to 9
to 19 observed targets (16 median) per full observing night.
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Number of allocated nights: The PI astronomer and her/his team would need 10 to 21 full observing nights to collect data
for ~ 200 objects. Assuming a weather-loss fraction of 0.25 (KAON 463), this requires 14 to 28 allocated nights (spread over
a few semester) to collect the needed sample of data.
Observing model: astronomers are requesting half to full night(s) for this science case in classical observing mode. The
astronomer(s) will be performing the observations remotely (either from Waimea or elsewhere) and assessing the data quality
on-the-fly. The observations require less than 1 mag of extinction in the V band (for the use of lasers). The PI and the science
team are responsible for the backup observing program.
3.2. Pre-observing planning:
This section presents the actions undertaken by the astronomers prior to the observations with emphasis on the use of the
NGAO planning tools.
-
Simulations: Astronomers will want to run a first iteration of simulation at the time of the proposal and estimate the
SNR per spatial and spectral resolution element assuming:
o A model for the galaxy (geometry, size and flux) provided by the astronomer.
o A 2-D PSF or an estimate for the SR, EE, provided by the NGAO planning tools.
o A exposure time calculator to get an estimate for the SNR that can be achieved.
Subsequent iterations for the simulations may take into account a more realistic geometry for the AO guide stars and
include other constrains such as the observing conditions (elevation range and an approximate seeing value)
NGS selection: The NGAO Natural Guide Star finder tool allows the astronomer to search for, extract and save
information for a few constellations of at least three natural guide stars. The information is retrieved from on-line or
local astronomical catalogs (USNO-B, GSC-II, SDSS). The planning tools helps the astronomer to register the AO
guide stars with respect to the science targets. The data will be saved and used for the acquisition at the telescope.
Most of the “legacy” high-z galaxy fields are well documented and have been surveyed at different wavelengths by
ground and space telescopes, e.g., GOODS North and South, Extended Groth strip, COSMOS, etc. For these cases, it
should be possible to extract the NGS location directly from these legacy surveys. One could also find and select
additional sources which intensity profile is similar to a point source (stellar fit parameters < 1) with the goal of
increasing the sky coverage for these areas. We plan to study this scenario during the PD and DD phases.
-
Observability: typical elevation range of the high-z fields for ~3 hours of observing?
-
Observing conditions: the conditions will need to be transparent (less than ~ 0.5 mag. of extinction at 589 nm - TBC)
for the use of lasers. In addition, the relative photometry should be better than 5% for the observations during a single
night (reqt #1.10).
3.3. AO observing mode:
The observations with the d-IFS will require the LGS AO mode with the medium to wide configuration for the LGS
asterism. The configuration for the LGS asterism will be optimized as a function of the location of the science targets for the
d-IFS and the location of the NGS. The planning tools will help the astronomer to select the LGS and NGS configuration
that optimizes an observational quantity (SR, EE or target selection)
The AO rotator will be in position angle mode: observers will set the orientation of the North axis, as projected on the d-IFS
for each observation of a set of targets.
In order to get an accurate estimate for the PSF, the astronomer will select to dedicate one of the d-IFS unit to observe a faint
star in the field, while brighter natural stars from the field will be used for the LOWFS and the truth WFS.
The observer may choose to observe a set of bright photometric or telluric calibrators with the d-IFS. We anticipate the use of
the d-IFS in NGS AO mode to maximize the observing efficiency (better SNR, minimal overhead).
3.4. Science instrument configuration:
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The science instrument configuration will be detailed during the Preliminary and Detailed Design phases for NGAO in
parallel to the studies for the d-IFS.
KAON 548 provide details for the d-IFS: a spaxel size of 70 milli-arcsec (2 pixels of 35 mas/spaxel), a field-of-view of ~ 1.0
x 3.0 arcseconds per units (#reqt 1.8). Six spectrograph units deployable over a field of regard of at least 120 arcseconds in
diameter.
3.5. Observing sequences:
This section describes the individual observing sequences
3.5.1. Acquisition
The science targets require to be centered on the science array with an accuracy of less than 10% of the field of view (#reqt
1.12) corresponding to 100 – 200 milli-arcsecond.
The targets to acquire during the acquisition are the three NGS for the LOWFS/TWFS and the astronomical sources for the dIFS. The d-IFS targets include galaxies plus maybe, simultaneous science field calibrators (point-like sources that can be
used to estimate the PSF, the telluric absorptions and/or the photometry). Subsequently, there are two main scenarios for this
science case:
a. Except for the 3 NGS, there are not point-like sources in the science field that can be used to check the d-IFS centering.
All science targets are faint and their final positioning will rely on the position from the literature and the system
pointing accuracy. This is a “blind acquisition & centering” scenario.
b. In addition to the 3 NGS, there are point-like sources in the science field that can be used to reference the centering for
the d-IFS (probe arms + MEMs + internal optics). The centering requirements can be loosen for this case at the expense
of the observing efficiency.
The NGAO acquisition is being designed to meet the requirement for case a). Yet we have included some time losses due to
re-centering in the estimation of the observing efficiency.
3.5.2. Science observing sequences
Several scenarios are anticipated for the science observing sequences:
a.
Dithering and micro-dithering without moving the telescope and opening the AO loops:
For this sequences, the observer will enter a set of n positions in instrument (x, y pixel or spaxels) or sky (RA, DEC
offsets) coordinates. The OSC Tools will be coordinating the sequences. Dithering without moving the telescope and
opening the loops minimizes the overhead, but it is restricted to small amplitude dither of less than 3 arcsecond if the
dithering is performed by the individual MEMs (See KAON 558). This allows the observer to recenter quickly the
reference objects on the d-IFS and possibly run independent dithering scripts for each IFU. A typical dithering script
will have the object positioned in two or more locations of the IFU, with minimum spatial overlap, allowing to record
the target and the sky on one IFU.
Need more information regarding micro-dithering (spaxel or sub-spaxel level).
We also anticipate moving the science probe arms independently for any move beyond the range of the MEMs. The
restrictions on the motion of the probe arms (depending on the deployment space and the variations in wavefront error)
is yet to be defined. While the field would stay registered, a subset of probe arms could be switching from targets to sky
(and targets to targets – TBC) within these constrains. In this scenario, the sky is recorded separately from the science
target.
The dither flexibility illustrated by these observing scenario might fit very well the case where sources of very different
brightness are observed (e.g., K=19 point-like source calibrator observed in parallel to a set of high-z galaxies).
b.
Offsetting:
Offsetting requires moving the telescope, pausing the AO loops (at least for the LOWFS/TWFS), repositioning the
LOWFS and LGS probe arms and resuming the AO loops. Offset will apply to all targets at once.
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We do anticipate to use the offset mode with d-IFS if a different set of targets are observed for the same science field.
This saves the time to re-acquire the NGS and perform a new LGS acquisition.
c.
Filter and instrument sequences
The d-IFS instrument will allow the observer to run different observing sequences such as filter, pixel, read modes, etc.
The observer should be able to set the priority for the instrument sequences with respect to the dithering sequences.
3.6. Science Calibrations:
- Flat-field and spectral calibrations:
Flat field and spectral calibrations are performed on the internal light source (integrating sphere) by the Observatory
support staff. The output of the calibrations is integrated in the rectification matrix, as part of the data reduction
pipeline. The requirements for these calibrations will be detailed during the study and design of the d-IFS.
- PSF calibrations:
Calibrating the PSF is critical to the quantitative analysis of the galaxies to derive e.g., the ensquared energy per spaxel.
This analysis is required per spectral channel; it is then required to estimate the PSF per spectral channel.
The quantitative requirements for the PSF calibrations have yet to be understood. Different methods are being assessed:
1) one IFU is used as a PSF monitoring, and/or 2) a model PSF is reconstructed from the telemetry (WFC and Cn^2
data). The first scenario is costly to science as it requires dedicating one probe arm to the observations of a point-like
source but provides a simultaneous PSF calibration for one location in the field. Extrapolating the PSF measured on one
location to any location in the corrected field has been demonstrated (Britton 2006). The second scenario still requires
some significant development and has yet to be demonstrated with LGS.
- Photometry
- Astrometry
3.7. Post-Observing
- Data Product
The generic data product includes:
- The raw science and calibration data
- The reduced science and calibration data
- The PSF reconstruction data from the WFC and Cn2 profiler telemetry, if applicable
- The image quality monitoring data (SR, EE, flux on LOWFS and laser return, fault events log, etc)
-
Data Reduction and Analysis
The d-IFS will include its own data reduction pipeline. The requirements for the DRP will be developed during the
design phase for the d-IFS.
-
Data archiving
The observatory will save and store at least one copy of the entire set of the data product, defined with the observer. The
requirements for the automated archive of the NGAO data will be studied and developed during the Preliminary Phase
for NGAO.
The archived data will be proprietary and the release mechanism for technical or scientific purpose after a certain delay
will be defined in the Preliminary Design phase of NGAO.
Backup science is treated as a different observing scenario.
4. Nearby Active Galactic Nuclei
5. Precision Astrometry: Measurements of General Relativity Effects in the Galactic Center
6. Imaging and characterization of extrasolar planets around nearby stars
Updated 7/13/2016 at 5:51 AM by D. Le Mignant
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Observing Scenarios with NGAO – Draft Version 1.0
7. Multiplicity of Minor Planets
8. QSO Host Galaxies
9. Gravitational Lensing
10. Astrometry Science in Sparse Fields
11. Resolved Stellar Populations in Crowded Fields
12. Debris Disks and Young Stellar Objects
13. Size, Shape and Composition of Minor Planets
14. Characterization of Gas Giant Planets
15. Characterization of Ice Giant Planets
16. Backup Science
Updated 7/13/2016 at 5:51 AM by D. Le Mignant
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